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Gaia Data Release 2: Observational Hertzsprung-Russell Diagrams ? Astronomy & Astrophysics manuscript no. DR2HRD c ESO 2018 August 14, 2018 Gaia Data Release 2: Observational Hertzsprung-Russell diagrams ? Gaia Collaboration, C. Babusiaux1; 2, F. van Leeuwen3, M.A. Barstow4, C. Jordi5, A. Vallenari6, D. Bossini6, A. Bressan7, T. Cantat-Gaudin6; 5, M. van Leeuwen3, A.G.A. Brown8, T. Prusti9, J.H.J. de Bruijne9, C.A.L. Bailer-Jones10, M. Biermann11, D.W. Evans3, L. Eyer12, F. Jansen13, S.A. Klioner14, U. Lammers15, L. Lindegren16, X. Luri5, F. Mignard17, C. Panem18, D. Pourbaix19; 20, S. Randich21, P. Sartoretti2, H.I. Siddiqui22, C. Soubiran23, N.A. Walton3, F. Arenou2, U. Bastian11, M. Cropper24, R. Drimmel25, D. Katz2, M.G. Lattanzi25, J. Bakker15, C. Cacciari26, J. Castañeda5, L. Chaoul18, N. Cheek27, F. De Angeli3, C. Fabricius5, R. Guerra15, B. Holl12, E. Masana5, R. Messineo28, N. Mowlavi12, K. Nienartowicz29, P. Panuzzo2, J. Portell5, M. Riello3, G.M. Seabroke24, P. Tanga17, F. Thévenin17, G. Gracia-Abril30; 11, G. Comoretto22, M. Garcia-Reinaldos15, D. Teyssier22, M. Altmann11; 31, R. Andrae10, M. Audard12, I. Bellas-Velidis32, K. Benson24, J. Berthier33, R. Blomme34, P. Burgess3, G. Busso3, B. Carry17; 33, A. Cellino25, G. Clementini26, M. Clotet5, O. Creevey17, M. Davidson35, J. De Ridder36, L. Delchambre37, A. Dell’Oro21, C. Ducourant23, J. Fernández-Hernández38, M. Fouesneau10, Y. Frémat34, L. Galluccio17, M. García-Torres39, J. González-Núñez27; 40, J.J. González-Vidal5, E. Gosset37; 20, L.P. Guy29; 41, J.-L. Halbwachs42, N.C. Hambly35, D.L. Harrison3; 43, J. Hernández15, D. Hestroffer33, S.T. Hodgkin3, A. Hutton44, G. Jasniewicz45, A. Jean-Antoine-Piccolo18, S. Jordan11, A.J. Korn46, A. Krone-Martins47, A.C. Lanzafame48; 49, T. Lebzelter50, W. Löffler11, M. Manteiga51; 52, P.M. Marrese53; 54, J.M. Martín-Fleitas44, A. Moitinho47, A. Mora44, K. Muinonen55; 56, J. Osinde57, E. Pancino21; 54, T. Pauwels34, J.-M. Petit58, A. Recio-Blanco17, P.J. Richards59, L. Rimoldini29, A.C. Robin58, L.M. Sarro60, C. Siopis19, M. Smith24, A. Sozzetti25, M. Süveges10, J. Torra5, W. van Reeven44, U. Abbas25, A. Abreu Aramburu61, S. Accart62, C. Aerts36; 63, G. Altavilla53; 54; 26, M.A. Álvarez51, R. Alvarez15, J. Alves50, R.I. Anderson64; 12, A.H. Andrei65; 66; 31, E. Anglada Varela38, E. Antiche5, T. Antoja9; 5, B. Arcay51, T.L. Astraatmadja10; 67, N. Bach44, S.G. Baker24, L. Balaguer-Núñez5, P. Balm22, C. Barache31, C. Barata47, D. Barbato68; 25, F. Barblan12, P.S. Barklem46, D. Barrado69, M. Barros47, S. Bartholomé Muñoz5, J.-L. Bassilana62, U. Becciani49, M. Bellazzini26, A. Berihuete70, S. Bertone25; 31; 71, L. Bianchi72, O. Bienaymé42, S. Blanco-Cuaresma12; 23; 73, T. Boch42, C. Boeche6, A. Bombrun74, R. Borrachero5, S. Bouquillon31, G. Bourda23, A. Bragaglia26, L. Bramante28, M.A. Breddels75, N. Brouillet23, T. Brüsemeister11, E. Brugaletta49, B. Bucciarelli25, A. Burlacu18, D. Busonero25, A.G. Butkevich14, R. Buzzi25, E. Caffau2, R. Cancelliere76, G. Cannizzaro77; 63, R. Carballo78, T. Carlucci31, J.M. Carrasco5, L. Casamiquela5, M. Castellani53, A. Castro-Ginard5, P. Charlot23, L. Chemin79, A. Chiavassa17, G. Cocozza26, G. Costigan8, S. Cowell3, F. Crifo2, M. Crosta25, C. Crowley74, J. Cuypersy34, C. Dafonte51, Y. Damerdji37; 80, A. Dapergolas32, P. David33, M. David81, P. de Laverny17, F. De Luise82, R. De March28, D. de Martino83, R. de Souza84, A. de Torres74, J. Debosscher36, E. del Pozo44, M. Delbo17, A. Delgado3, H.E. Delgado60, S. Diakite58, C. Diener3, E. Distefano49, C. Dolding24, P. Drazinos85, J. Durán57, B. Edvardsson46, H. Enke86, K. Eriksson46, P. Esquej87, G. Eynard Bontemps18, C. Fabre88, M. Fabrizio53; 54, S. Faigler89, A.J. Falcão90, M. Farràs Casas5, L. Federici26, G. Fedorets55, P. Fernique42, F. Figueras5, F. Filippi28, K. Findeisen2, A. Fonti28, E. Fraile87, M. Fraser3; 91, B. Frézouls18, M. Gai25, S. Galleti26, D. Garabato51, F. García-Sedano60, A. Garofalo92; 26, N. Garralda5, A. Gavel46, P. Gavras2; 32; 85, J. Gerssen86, R. Geyer14, P. Giacobbe25, G. Gilmore3, S. Girona93, G. Giuffrida54; 53, F. Glass12, M. Gomes47, M. Granvik55; 94, A. Gueguen2; 95, A. Guerrier62, J. Guiraud18, R. 22 2 85; 32 11; 10 2 46 75 arXiv:1804.09378v2 [astro-ph.SR] 13 Aug 2018 Gutiérrez-Sánchez , R. Haigron , D. Hatzidimitriou , M. Hauser , M. Haywood , U. Heiter , A. Helmi , J. Heu2, T. Hilger14, D. Hobbs16, W. Hofmann11, G. Holland3, H.E. Huckle24, A. Hypki8; 96, V. Icardi28, K. Janßen86, G. Jevardat de Fombelle29, P.G. Jonker77; 63, Á.L. Juhász97; 98, F. Julbe5, A. Karampelas85; 99, A. Kewley3, J. Klar86, A. Kochoska100; 101, R. Kohley15, K. Kolenberg102; 36; 73, M. Kontizas85, E. Kontizas32, S.E. Koposov3; 103, G. Kordopatis17, Z. Kostrzewa-Rutkowska77; 63, P. Koubsky104, S. Lambert31, A.F. Lanza49, Y. Lasne62, J.-B. Lavigne62, Y. Le Fustec105, C. Le Poncin-Lafitte31, Y. Lebreton2; 106, S. Leccia83, N. Leclerc2, I. Lecoeur-Taibi29, H. Lenhardt11, F. Leroux62, S. Liao25; 107; 108, E. Licata72, H.E.P. Lindstrøm109; 110, T.A. Lister111, E. Livanou85, A. Lobel34, M. López69, S. Managau62, R.G. Mann35, G. Mantelet11, O. Marchal2, J.M. Marchant112, M. Marconi83, S. Marinoni53; 54, G. Marschalkó97; 113, D.J. Marshall114, M. Martino28, G. Marton97, N. Mary62, D. Massari75, G. Matijevicˇ86, T. Mazeh89, P.J. McMillan16, S. Messina49, D. Michalik16, N.R. Millar3, D. Molina5, R. Molinaro83, Article number, page 1 of 28 A&A proofs: manuscript no. DR2HRD L. Molnár97, P. Montegriffo26, R. Mor5, R. Morbidelli25, T. Morel37, D. Morris35, A.F. Mulone28, T. Muraveva26, I. Musella83, G. Nelemans63; 36, L. Nicastro26, L. Noval62, W. O’Mullane15; 41, C. Ordénovic17, D. Ordóñez-Blanco29, P. Osborne3, C. Pagani4, I. Pagano49, F. Pailler18, H. Palacin62, L. Palaversa3; 12, A. Panahi89, M. Pawlak115; 116, A.M. Piersimoni82, F.-X. Pineau42, E. Plachy97, G. Plum2, E. Poggio68; 25, E. Poujoulet117, A. Prša101, L. Pulone53, E. Racero27, S. Ragaini26, N. Rambaux33, M. Ramos-Lerate118, S. Regibo36, C. Reylé58, F. Riclet18, V. Ripepi83, A. Riva25, A. Rivard62, G. Rixon3, T. Roegiers119, M. Roelens12, M. Romero-Gómez5, N. Rowell35, F. Royer2, L. Ruiz-Dern2, G. Sadowski19, T. Sagristà Sellés11, J. Sahlmann15; 120, J. Salgado121, E. Salguero38, N. Sanna21, T. Santana-Ros96, M. Sarasso25, H. Savietto122, M. Schultheis17, E. Sciacca49, M. Segol123, J.C. Segovia27, D. Ségransan12, I-C. Shih2, L. Siltala55; 124, A.F. Silva47, R.L. Smart25, K.W. Smith10, E. Solano69; 125, F. Solitro28, R. Sordo6, S. Soria Nieto5, J. Souchay31, A. Spagna25, F. Spoto17; 33, U. Stampa11, I.A. Steele112, H. Steidelmüller14, C.A. Stephenson22, H. Stoev126, F.F. Suess3, J. Surdej37, L. Szabados97, E. Szegedi-Elek97, D. Tapiador127; 128, F. Taris31, G. Tauran62, M.B. Taylor129, R. Teixeira84, D. Terrett59, P. Teyssandier31, W. Thuillot33, A. Titarenko17, F. Torra Clotet130, C. Turon2, A. Ulla131, E. Utrilla44, S. Uzzi28, M. Vaillant62, G. Valentini82, V. Valette18, A. van Elteren8, E. Van Hemelryck34, M. Vaschetto28, A. Vecchiato25, J. Veljanoski75, Y. Viala2, D. Vicente93, S. Vogt119, C. von Essen132, H. Voss5, V. Votruba104, S. Voutsinas35, G. Walmsley18, M. Weiler5, O. Wertz133, T. Wevers3; 63, Ł. Wyrzykowski3; 115, A. Yoldas3, M. Žerjal100; 134, H. Ziaeepour58, J. Zorec135, S. Zschocke14, S. Zucker136, C. Zurbach45, and T. Zwitter100 (Affiliations can be found after the references) Received ; accepted ABSTRACT Context. Gaia Data Release 2 provides high-precision astrometry and three-band photometry for about 1.3 billion sources over the full sky. The precision, accuracy, and homogeneity of both astrometry and photometry are unprecedented. Aims. We highlight the power of the Gaia DR2 in studying many fine structures of the Hertzsprung-Russell diagram (HRD). Gaia allows us to present many different HRDs, depending in particular on stellar population selections. We do not aim here for completeness in terms of types of stars or stellar evolutionary aspects. Instead, we have chosen several illustrative examples. Methods. We describe some of the selections that can be made in Gaia DR2 to highlight the main structures of the Gaia HRDs. We select both field and cluster (open and globular) stars, compare the observations with previous classifications and with stellar evolutionary tracks, and we present variations of the Gaia HRD with age, metallicity, and kinematics. Late stages of stellar evolution such as hot subdwarfs, post-AGB stars, planetary nebulae, and white dwarfs are also analysed, as well as low-mass brown dwarf objects. Results. The Gaia HRDs are unprecedented in both precision and coverage of the various Milky Way stellar populations and stellar evolutionary phases. Many fine structures of the HRDs are presented. The clear split of the white dwarf sequence into hydrogen and helium white dwarfs is presented for the first time in an HRD. The relation between kinematics and the HRD is nicely illustrated. Two different populations in a classical kinematic selection of the halo are unambiguously identified in the HRD. Membership and mean parameters for a selected list of open clusters are provided. They allow drawing very detailed cluster sequences, highlighting fine structures, and providing extremely precise empirical isochrones that will lead to more insight in stellar physics. Conclusions. Gaia DR2 demonstrates the potential of combining precise astrometry and photometry for large samples for studies in stellar evolution and stellar population and opens an entire new area for HRD-based studies. Key words. parallaxes – Hertzsprung-Russell and C-M diagrams – solar neighbourhood – Stars: evolution 1. Introduction geneous samples that cover the full HRD. Moreover, a precise HRD provides a great framework for exploring stellar popula- The Hertzsprung-Russell diagram (HRD) is one of the most im- tions and stellar systems. portant tools in stellar studies. It illustrates empirically the rela- tionship between stellar spectral type (or temperature or colour Up to now, the most complete solar neighbourhood empir- index) and luminosity (or absolute magnitude). The position of ical HRD could be obtained by combining the Hipparcos data a star in the HRD is mainly given by its initial mass, chemical (Perryman et al. 1995) with nearby stellar catalogues to provide composition, and age, but effects such as rotation, stellar wind, the faint end (e.g.
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